Neutrino Parameters

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Neutrino Parameters
NNN05 Next Generation of Nucleon Decay and
Neutrino Detectors
Aussois (Savoie) 7-9 April 2005
G. L. FogliDipartimento di Fisica INFNBari,
Italy
Mainly based on work done in collaboration with
E. Lisi, A. Marrone, A. Melchiorri, A. Mirizzi,
D. Montanino, A. Palazzo, A.M. Rotunno, P. Serra,
J. Silk
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Outline
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3n mass-mixing parameters notation,
conventions, remarks
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3n mixing notation, conventions, remarks
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3n masses notation, conventions, remarks
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3n Majorana phases notation, conventions, remarks
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Constraints on (Dm2, sin2q23, sin2q13) from
SKK2KCHOOZ
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SK constraints on (Dm2, sin2q23) at sin2q13 0
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SK and K2K constraints on (Dm2, sin2q23) at
sin2q13 0
A joint, official SK K2K combination would be
desirable (note that interaction and detection
systematics are similar and correlated in SK and
K2K).
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Constraints on (Dm2, sin2q23) adding CHOOZ, with
sin2q13 unconstrained
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Constraints on (Dm2, sin2q23, sin2q13) from SK
K2K CHOOZ
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Constraints on (dm2, sin2q12, sin2q13) from
solar neutrinos KamLAND
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Historical notes
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in 2004 at q13 0
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What about MSW effects in the Sun ?
( a way of measuring GF through solar
neutrino oscillations )
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2005 (last month)
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3n analysis of 2004 solar KamLAND data (q13
free)
SNO 2005 data not included
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Grand Total from global analysis of
oscillation data
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Marginalized Dc2 curves for each parameter
(2004)
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Numerical 2s ranges (95 CL for 1 dof), 2004
data
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Probing absolute n masses through
non-oscillation searches
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Three main tools,
identified with three observables sensitive to
absolute n masses
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Constraints from oscillation data only
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Input from Tritium b-decay experiments
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Input from Germanium 0n2b-decay experiments
From the available estimates of the nuclear
matrix elements with their uncertainties one can
derive an estimate of the effective Majorana
mass. However, since the claim from
Heidelberg-Moscow has been subject to criticism,
in the following, we assume two possible 0n2b
inputs for the global analysis (1s error)
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Constraint on S from cosmological data
Likelihood distribution for S from joint analysis
of several data sets. No evidence for a n mass
and upper bounds depending on several inputs and
priors. In particular

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Adding upper bounds from laboratory and cosmology
The cosmological upper limit on S formally
dominates over the lab upper limits on mb and mbb
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Adding lower bounds on mbb from the claimed 0n2b
signal
However, the global allowed region extends
somewhat outside the 2s limits from cosmology and
0n2b data separately a clear indication of some
tension between the two sets of data.
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Adding Lyman-a forest to cosmological data
This modifies the upper limit on S, improved by a
factor 3.
A. 0n2b claim rejected
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B. 0n2b claim accepted
The absence of overlap is a clear symptom of
problems either in some data or in the
theoretical interpretation, and prevents any
global combination of data. However
It is premature to conclude that the 0n2b claim
is ruled out by cosmological data
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Galactic SN and Next generation of Nucleon decay
and Neutrino detectors
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NNN detectors and galactic SN
Two of the currently unknown parameters,
sign(Dm2) and q13, might be accessed in a large
scale (e.g. 0.4 Mton) Cherenkov detector through
their effect on supernova n oscillations.
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Neutrino crossing probability
On the basis of the shock wave profiles, the n
crossing probability PH(t) can be estimated for
representatives values of sin2q13 and fixed En.
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Signatures of shock wave effects
An analysis of the absolute time spectra shows
that the signatures of shock wave effects can be
enhanced by comparing time spectra at different
energies.
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Signatures of shock wave effects
An analysis of the absolute time spectra shows
that the signatures of shock wave effects can be
enhanced by comparing time spectra at different
energies.

forwardreverse shock waves
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Conclusions
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This workshop
certainly help us to
better understand how NNN detectors can
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Input from cosmological data
Joint analysis of several data sets. In
particular, the following data set have been
considered